Cosmological Inflation and the Primordial Power Spectrum

Mathematics – Logic

Scientific paper

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Scientific paper

In this thesis, we discuss two important aspects of cosmological inflation, which is a prominent part of modern cosmology. Since inflation typically occurs at ultrahigh energy scales, string theory is a popular framework to achieve inflation. We investigate the fine-tuning problem in string theoretic inflation models, based on a brane-antibrane potential. We phenomenologically quantify the degree of fine-tuning by defining an effective volume in the part of parameter space which is consistent with observational constraints. Moreover, we use Monte Carlo methods to illustrate that the degree of fine-tuning can be substantially alleviated. We also explore a novel mechanism of dynamical tuning of a flat potential in brane-antibrane inflation. Because of competing effects between its interactions with D7-branes and D3-branes, a stack of D3-branes gives rise to a local minimum in the potential. As branes successively tunnel out, the potential barrier is eventually replaced by a flat inflection point, around which the remaining branes easily inflate. We give an example where this time-dependent flattening of the inflaton potential is possible. Another important aspect of inflation is the primordial power spectrum. In this thesis, we consider a primordial power spectrum with a k 3 component, which can be generated through different mechanisms and is a good representative of the generic spikelike features. We explore the possibility that the features could be observably large. Although there is no strong evidence, large spikes are not ruled out by the data, and we give constraints on the k3 component.

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